期刊
PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA
卷 113, 期 15, 页码 3944-3949出版社
NATL ACAD SCIENCES
DOI: 10.1073/pnas.1522363113
关键词
neutron stars; magnetars; pulsars; magnetohydrodynamics
资金
- Science and Technology Funding Council (STFC) [ST/K000853/1]
- STFC
- STFC [ST/H008802/1, ST/N000676/1, ST/K000853/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K000853/1, ST/N000676/1, ST/H008802/1] Funding Source: researchfish
Current models of magnetars require extremely strong magnetic fields to explain their observed quiescent and bursting emission, implying that the field strength within the star's outer crust is orders of magnitude larger than the dipole component inferred from spin-down measurements. This presents a serious challenge to theories of magnetic field generation in a proto-neutron star. Here, we present detailed modeling of the evolution of the magnetic field in the crust of a neutron star through 3D simulations. We find that, in the plausible scenario of equipartition of energy between global-scale poloidal and toroidal magnetic components, magnetic instabilities transfer energy to nonaxisymmetric, kilometer-sized magnetic features, in which the local field strength can greatly exceed that of the global-scale field. These intense small-scale magnetic features can induce high-energy bursts through local crust yielding, and the localized enhancement of Ohmic heating can power the star's persistent emission. Thus, the observed diversity in magnetar behavior can be explained with mixed poloidal-toroidal fields of comparable energies.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据